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%% Rob Beswick
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%% Dr Rob Beswick |
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& \multicolumn{1}{|c|}{\large\em An electronic publication dedicated to}\\ [0.3cm]
\multicolumn{1}{|l|}{\hspace{0.5cm}\LARGE\bf\sf Galaxies} & \multicolumn{1}{|c|}{\large\em the observation and theory of}\\ [0.3cm]
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\multicolumn{1}{|c|}{\large\bf\sf No. 105 --- December 2005 } &
\multicolumn{1}{|c|}{\bf\sf Editor: Rob Beswick (rb@ast.man.ac.uk)} \\ [-0.1cm]
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{\Large\em Abstracts - Thesis Abstracts - Jobs - Meetings}
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\begin{center}
{\Large\sf From the Editor}
\end{center}
\vspace*{0.6cm}
The Active Galaxies Newsletter is produced monthly. The deadline for
contributions is the last friday of the month. The Latex macros for
submitting abstracts and dissertation abstracts are appended to each
issue of the newsletter and are also available on the web page.
\newline Rob Beswick
\vspace*{1cm}
\begin{center}
{\Large\sf Abstracts of recently accepted papers}
\end{center}
\vspace*{0.6cm}
\vspace*{0.6cm}
{\large\bf{ AGNs and Starbursts: What Is the Real Connection?}}
{\bf{Luis C. Ho$^1$ }}
$^1$ {The Observatories of the Carnegie Institution of Washington, 813
Santa Barbara St., Pasadena, CA 91101}
\newcommand{\oii}{[\ion{O}{2}]}
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{
It is now widely believed that the growth of massive black holes is
closely linked to the formation of galaxies, but there have been few
concrete constraints on the actual physical processes responsible for
this coupling. Investigating the connection between AGN and starburst
activity may offer some empirical guidance on this problem. I summarize
previous observational searches for young stars in active galaxies,
concluding that there is now compelling evidence for a significant
post-starburst population in many luminous AGNs, and that a direct,
causal link may exist between star formation and black hole accretion.
Quantifying the ongoing star formation rate in AGNs, however, is much
more challenging because of the strong contamination by the active
nucleus. I discuss recent work attempting to measure the star formation
rate in luminous AGNs and quasars. The exceptionally low level of coeval
star formation found in these otherwise gas-rich systems suggests that
the star formation efficiency in the host galaxies is suppressed in the
presence of strong AGN feedback.}
{Invited review to appear in {\it Extreme Starbursts: Near and Far}.}
{E-mail contact: lho@ociw.edu,\newline preprint available at
http://xxx.lanl.gov/abs/astro-ph/0511157}
\vspace*{0.6cm}
{\large\bf{The soft X--ray/NLR connection: a single photoionized medium?}}
{\bf{ Stefano Bianchi$^1$, Matteo Guainazzi$^1$, Marco Chiaberge$^2$ $^3$}}
$^1$ {XMM-Newton Science Operations Center, European Space Astronomy
Center, ESA, Apartado 50727, E-28080 Madrid, Spain} \\
$^2$ {Space Telescope Science Institute, 3700 San Martin Drive,
Baltimore, MD 21218} \\
$^3$ {INAF-Istituto di Radioastronomia, Via P. Gobetti 101, 40129
Bologna, Italy}
{We present a sample of 8 nearby Seyfert 2 galaxies observed by
\textit{HST} and \textit{Chandra}. All of the sources present soft X-ray
emission which is coincident in extension and overall morphology with the
[{O\,\textsc{iii}}] emission. The spectral analysis reveals that the soft
X-ray emission of all the objects is likely to be dominated by a
photoionized gas. This is strongly supported by the 190 ks combined
XMM-\textit{Newton}/RGS spectrum of Mrk~3, which different diagnostic
tools confirm as bei ng produced in a gas in photoionization equilibrium
with an important contribution from resonant scattering. We tested with
the code \textsc{cloudy} a simple scenario where the same gas
photoionized by the nuclear continuum produces both the soft X-ray a nd
the [{O\,\textsc{iii}}] emission. Solutions satisfying the observed ratio
between the two components exist, and require the density to decrease
with radius roughly like $r^{-2}$, similarly to what often found for the
Narrow Line Region.}
{ Accepted by A\&A }
{E-mail contact: Stefano.Bianchi@sciops.esa.int,\newline preprint
available at http://es.arxiv.org/abs/astro-ph/0511216}
\vspace*{0.6cm}
{\large\bf{Revisiting the Infrared Spectra of Active Galactic Nuclei with
a New Torus Emission Model}}
{\bf{ J. Fritz$^{1,2}$, A. Franceschini$^1$ and E. Hatziminaoglou$^2$ }}
$^1$ {Dipartimento di Astronomia, Vicolo Osservatorio 2, I-35122 Padova,
Italy}\\
$^2$ {Instituto de Astrof\'{i}sica de Canarias, C/ V\'{i}a L\'{a}ctea
s/n, E-38200 La Laguna, Spain}
{We describe improved modelling of the emission by dust in a
toroidal--like structure heated by a central illuminating source within
Active Galactic Nuclei (AGN). We chose a simple but realistic torus
geometry, a flared disc, and a dust grain distribution function including
a full range of grain sizes. The optical depth within the torus is
computed in detail taking into account the different sublimation
temperatures of the silicate and graphite grains, which solves previously
reported inconsistencies in the silicate emission feature in type-1 AGN.
We exploit this model to study the spectral energy distributions (SEDs)
of $58$ extragalactic (both type-1 and type-2) sources using archival
optical and infrared (IR) data. We find that both AGN and starburst
contributions are often required to reproduce the observed SEDs, although
in a few cases they are very well fitted by a pure AGN component. The AGN
contribution to the far-IR luminosity is found to be higher in type-1
sources, with all the type-2 requiring a substantial contribution from a
circum-nuclear starburst. Our results appear in agreement with the AGN
Unified Scheme, since the distributions of key parameters of the torus
models turn out to be compatible for type-1 and type-2 AGN. Further
support to the unification concept comes from comparison with
medium-resolution IR spectra of type-1 AGN by the Spitzer observatory,
showing evidence for a moderate silicate emission around $10 \mu$ which
our code reproduces. >From our analysis we infer accretion flows in the
inner nucleus of local AGN characterized by high equatorial optical
depths ($A_V\simeq 100$), moderate sizes ($R_{max}<100\ pc$) and very
high covering factors ($f\simeq 80$ per cent) on average.}
{ Accepted by MNRAS}
{E-mail contact: fritz@pd.astro.it,\newline preprint available at
http://xxx.lanl.gov/abs/astro-ph/0511428}
\vspace*{0.6cm}
{\large\bf{Photoionized H$\beta$ Emission in NGC 5548: It Breathes!}}
{\bf{Edward M. Cackett$^1$, Keith Horne$^1$}}
$^1$ {School of Physics and Astronomy,
University of St.~Andrews,
KY16 9SS, Scotland, UK}
{Emission-line regions in active galactic nuclei and other photoionized
nebulae should become larger in size when the ionizing luminosity
increases. This ``breathing'' effect is observed for the H$\beta$
emission in NGC~5548 by using H$\beta$ and optical continuum lightcurves
from the 13-year 1989-2001 AGN~Watch monitoring campaign. To model the
breathing, we use two methods to fit the observed lightcurves in detail:
(i) parameterized models and, (ii) the \texttt{MEMECHO} reverberation
mapping code. Our models assume that optical continuum variations track
the ionizing radiation, and that the H$\beta$ variations respond with
time delays $\tau$ due to light travel time. By fitting the data using a
delay map $\Psi(\tau,F_c)$ that is allowed to change with continuum flux
$F_c$, we find that the strength of the H$\beta$ response decreases and
the time delay increases with ionizing luminosity. The parameterized
breathing models allow the time delay and the H$\beta$ flux to depend on
the continuum flux so that, $\tau \propto F_c^{\beta}$ and $F_{H\beta}
\propto F_c^{\alpha}$. Our fits give $0.1 < \beta < 0.46$ and $0.57 <
\alpha < 0.66$. $\alpha$ is consistent with previous work by Gilbert \&
Peterson (2003) and Goad, Korista and Knigge (2004). Although we find
$\beta$ to be flatter than previously determined by Peterson
et~al.~(2002) using cross-correlation methods, it is closer to the
predicted values from recent theoretical work by Korista \& Goad (2004).}
{ Accepted by MNRAS }
{E-mail contact: emc14@st-and.ac.uk,\newline preprint available at
http://arxiv.org/abs/astro-ph/0510800}
\newpage
%\vspace*{0.6cm}
{\large\bf{ The bulk Lorentz factor crisis of T\lowercase{e}V blazars :
evidence for an inhomogeneous pileup energy distribution ?}}
{\bf{Gilles Henri$^1$ and Ludovic Saug\'e$^2$}}
$^1$ {Laboratoire d'Astrophysique de Grenoble, Universit\'e
Joseph-Fourier, BP~53, F-38041 Grenoble, France} \\
$^2$ {Institut de Physique Nucl\'eaire de Lyon, UCBL/IN2P3-CNRS ,
4, rue Enrico Fermi, F-69622, Villeurbanne cedex, France}
{There is growing evidence that the estimations of the beaming Doppler
factor in TeV BL Lac object based on the Self Synchrotron Compton (SSC)
models are in strong disagreement with those deduced from the unification
models between blazars and radio galaxies. When corrected from
extragalactic absorption by the diffuse infrared background (DIrB), the
SSC one-zone models require very high Lorentz factor (around 50) to avoid
strong $\gamma-\gamma$ absorption. However, the statistics on beamed
\textit{vs.} unbeamed objects, as well as the luminosity contrast, favors
much lower Lorentz factor of the order of 3. In this paper, we show that
for the special case of Markarian 501, the need for very high Lorentz
factor is unavoidable for all one- zone models where all photons are
assumed to be produced at the same location at the same time. Models
assuming a double structure with two different beaming patterns can
partially solve the problem of luminosity contrast, but we point out that
they are inconsistent with the statistics on the number of detected TeV
sources. The only way to solve the issue is to consider inhomogeneous
models, where low energy and high energy photons are not produced at the
same place, allowing for much smaller Lorentz factors. It implies that
the jet is stratified, but also that the particle energy distribution is
close to a monoenergetic one, and that pair production is likely to be
significant. The implications on relativistic jet physics and particle
acceleration mechanism are discussed.}
{ Accepted for publication in the Astrophysical Journal }
{E-mail contact: Gilles.Henri@obs.ujf-grenoble.fr or
Ludovic.Sauge@obs.ujf-grenoble.fr,\newline preprint available at
http://arxiv.org/abs/astro-ph/0511610}
\vspace*{0.6cm}
{\large\bf{Long-term variability of the optical emission lines in the
nuclear spectrum of the Seyfert galaxy NGC 3227}}
{\bf{ I.Pronik$^1$, L.Metik$^1$ }}
$^1$ {Crimean Astrophysical Observatory, Nauchny, Crimea, Ukraine; Isaac
Newton Institute of Chile, Crimean Branch, Ukraine}
{53 spectrograms in the optical region (3700-7300 \AA) with the spectral
resolution $\sim$ 8\AA have been obtained for the Seyfert nucleus of the
galaxy NGC 3227 with the 6-m telescope on 1977 January while the nucleus
was in the historically important epoch of its extreme maximum
brightness. Width of the slit was 1$''$, length of the box during the
spectra measurements was 1.5$''$. Data obtained by us and those compiled
from literature showed that profiles of the Balmer lines H$\alpha$,
H$\beta$ and H$\gamma$ are different evidencing that the gas emitting
these lines is highly self-absorbed. It was shown that narrow components
of the profiles revealed by Rubin and Ford kept their positions (radial
velocities) over 25 years. The components showed intensity variations
compare to the central one from minimum to maximum of the nucleus
brightness. The same variations were observed by us earlier in the
emission line profiles of the NGC 7469 nucleus spectrum. Narrow profile
components can reflect long-lived flows or jets in the broad line region
(BLR). Obtained facts evidenced that long-lived gas streams and flows
causing narrow components of broad line profiles presented not only when
BLR of accretion disc is strong but when BLR of accretion disc declined.
Blue bump at radial velocity of -5000 km/s in H$\gamma$ profile was
revealed in spectra of high states of the nucleus, which disappeared in
low state. One of the interpretations of this event can be in the
framework of a model of one-sided or two-sided gas ejection during the
high state of the nucleus, positive radial velocities of which being
screened out by a circumnuclear disk.}
{ Accepted by Astrphysics and Space Science }
{E-mail contact: ipronik@crao.crimea.ua}
\vspace*{0.6cm}
{\large\bf{The supermassive black hole in Centaurus A:\\ a benchmark for
gas kinematical measurements}}
{\bf{ A.~Marconi$^1$, G.~Pastorini$^2$, F.~Pacini$^2$,
D.~J.~Axon$^{3,4}$, A.~Capetti$^5$, D.~Macchetto$^{6,7}$,
A.~M.~Koekemoer$^6$ \ and E.~J.~Schreier$^8$ }}
$^1$ {INAF - Osservatorio Astrofisico di Arcetri Largo E. Fermi 5,
I-50125 Firenze, Italy} \\
$^2$ {Dipartimento di Astronomia e Scienza dello Spazio, Universit\`a
degli Studi di Firenze Largo E. Fermi 2, I-50125 Firenze, Italy} \\
$^3$ {Department of Physics, Rochester Institute of Technology, 85 Lomb
Memorial Drive, Rochester, NY 14623, USA} \\
$^4$ {Department of Physical Sciences, University of Hertfordshire,
Hatfield AL10 9AB, UK} \\
$^5$ {INAF - Osservatorio Astronomico di Torino, Strada Osservatorio
20, I-10025 Pino Torinese, Italy} \\
$^6$ {Space Telescope Science Institute 3700 San Martin Drive,
Baltimore, MD 21218, USA} \\
$^7$ {Affiliated with ESA's Space Telescope Division} \\
$^8$ {Associated Universities, Inc. Suite 730 1400 16th Street, NW
Washington, DC 20036, USA} \\
\newcommand{\MBH}{\ensuremath{M_\mathrm{BH}}}
\newcommand{\Msun}{\ensuremath{\mathrm{M}_\odot}}
\newcommand{\xten}[1]{\times\ensuremath{10^{#1}}}
{We present new HST Space Telescope Imaging Spectrograph observations
of the nearby radio galaxy NGC 5128 (Centaurus A). The bright emission
line with longest wavelength accessible from HST, [SIII]$\lambda
9533$\AA, was used to study the kinematics of the ionized gas in the
nuclear region with a 0.1" spatial resolution. The STIS data were
analized in conjunction with the ground-based near-infrared Very Large
Telescope ISAAC spectra used by Marconi et al.~2001 to infer the
presence of a supermassive black hole and measure its mass. The two
sets of data have spatial resolutions differing by almost a factor of
five but provide independent and consistent measures of the BH mass,
which are in agreement with our previous estimate based on the ISAAC
data alone. The gas kinematical analysis provides a mass of
$\MBH=(1.1\pm0.1)\xten{8}\Msun$ for an assumed disk inclination of
$i=25$ deg or $\MBH= (6.5\pm0.7)\xten{7}\Msun$ for $i=35$ deg, the
largest $i$ value allowed by the data. We performed a detailed analysis
of the effects on \MBH\ of the intrinsic surface brightness
distribution of the emission line, a crucial ingredient in the gas
kinematical analysis. We estimate that the associated systematic errors
are no larger than $0.08$ in $\log\MBH$, comparable with statistical
errors and indicating that the method is robust. However, the intrinsic
surface brightness distribution has a large impact on the value of the
gas velocity dispersion. A mismatch between the observed and model
velocity dispersion is not necessarily an indication of non-circular
motions or kinematically hot gas, but is as easily due to an inaccurate
computation arising from too course a model grid, or the adoption of an
intrinsic brightness distribution which is too smooth. The observed
velocity dispersion in our spectra can be matched with a circularly
rotating disk and also the observed line profiles and the higher order
moments in the Hermite expansion of the line profiles, $h_3$ and $h_4$,
are consistent with emission from such a disk. To our knowledge,
Centaurus A is the first external galaxy for which reliable BH mass
measurements from gas and stellar dynamics are available and, as in the
case of the Galactic Center, the \MBH\ gas kinematical estimate is in
good agreement with that from stellar dynamics. The BH mass in
Centaurus A is in excellent agreement with the correlation with
infrared luminosity and mass of the host spheroid but is a factor $\sim
2-4$ above the one with the stellar velocity dispersion. But this
disagreement is not large if one takes into account the intrinsic
scatter of the $\MBH-\sigma_\mathrm{e}$ correlation. Finally, the high
HST spatial resolution allows us to constrain the size of any cluster
of dark objects alternative to a BH to $r_\bullet<0.035"$ ($\simeq 0.6$
pc). Thus Centaurus A ranks among the best cases for supermassive
Black Holes in galactic nuclei.}
{ Accepted by Astronomy \& Astrophysics }
{E-mail contact: marconi@arcetri.astro.it,\newline preprint available at
http://arxiv.org/abs/astro-ph/0507435}
\vspace*{0.6cm}
{\large\bf{Stellar populations in a complete sample of local radio
galaxies}}
{\bf{ D.~Raimann$^{1,2}$, T.~Storchi-Bergmann$^1$, H.~Quintana$^3$,
R.~Hunstead$^4$ \ and L.~Wisotzki$^5$ }}
$^1$ {Instituto de F\'{\i}sica, Universidade Federal do Rio Grande do
Sul, CP15051, Porto Alegre. 91501-970, RS, Brazil}\\
$^2$ {Universidade do Estado de Santa Catarina -- CEO, Rua Arcaj\'u
s/n, Pinhalzinho, 89870-000, SC, Brazil} \\
$^3$ {Facultad de F\'{\i}sica, Pontificia Universitad Catolica de
Chile, Santiago, Chile} \\
$^4$ {School of Physics, University of Sydney, NSW 2006, Australia} \\
$^5$ {Astrophysikalisches Institut Potsdam, Potsdam, Germany}
{We investigate the nature of the continuum emission and stellar
populations in the inner 1--3 kiloparsecs of a complete sample of
twenty-four southern radio galaxies, and compare the results with a
control sample of eighteen non-active early-type galaxies. Twelve of
the radio galaxies are classified as Fanaroff-Riley type I (FR\,I),
eight as FR\,II and four as intermediate or undefined type (FR\,x).
Optical long-slit spectra are used to perform spectral synthesis as a
function of distance from the nucleus at an average sampling of
0.5--1.0\,kpc and quantify the relative contributions of a blue
featureless continuum and stellar population components of different
ages. Our main finding is a systematic difference between the stellar
populations of the radio and control sample galaxies: the former have a
larger contribution from an intermediate age (1\,Gyr) component,
suggesting a connection between the present radio activity and a
starburst which occurred $\sim$1\,Gyr ago. In addition, we find a
correlation between the contribution of the 1\,Gyr component and the
radio power, suggesting that more massive starbursts have led to more
powerful radio emission. A similar relation is found between the radio
power and the mean age of the stellar population, in the sense that
stronger nuclear activity is found in younger galaxies. We also find
that the stellar populations of FR\,I galaxies are, on average, older
and more homogeneous than those of FR\,IIs. Significant population
gradients were found in only four radio galaxies, which are also those
with more than 10\,\% of their total flux at 4020\,\AA\ contributed by
age components younger than 100\,Myr and/or a featureless continuum
(indistinguishable from a 3\,Myr old stellar population).}
{ Accepted by MNRAS. }
{E-mail contact: raimann@if.ufrgs.br,\newline preprint available at
astro-ph/0510818}
\newpage
%\vspace*{0.6cm}
{\large\bf{The dust-eliminated shape of quasar spectra in the
near-infrared: a hidden part of the big blue bump}}
{\bf{ Makoto Kishimoto$^1$, Robert Antonucci$^2$ \ and Omer Blaes$^2$ }}
$^1$ {Institute for Astronomy, University of Edinburgh, Blackford Hill,
Edinburgh EH9 3HJ, UK} \\
$^2$ {Physics Department, University of California, Santa Barbara, CA
93106, USA}
{The near-infrared shape of the big blue bump component in quasar
spectra has been essentially unknown. It usually cannot be observed
directly, due to the strong hot dust emission which dominates quasar
spectra longward of $\sim$1$\mu$m. However this is quite an important
part of the spectrum theoretically. At least bare disk models provide
quite a robust prediction for the overall continuum shape in the
near-infrared. Self-gravity should become important in the outer,
near-infrared emitting regions of the putative disk, possibly leaving a
signature of disk truncation in the near-infrared. We propose here
that this important part of the spectrum can be revealed for the first
time by observing polarized flux from normal quasars. At least in some
polarized quasars, the emission lines are all unpolarized and so the
polarized flux should originate interior to the broad line region, and
therefore also interior to the dust emitting region. This can then be
used to eliminate the dust emission. We present the results of
near-infrared polarimetry for such three quasars (Ton202, 4C37.43, B2
1208+32). The data for Ton202 have the highest S/N, and the
near-infrared polarized flux in this case is measured to have quite a
blue shape, $F_{\nu} \propto \nu^{+0.42\pm0.29}$, intriguingly
consistent with the simple multi-temperature black body, bare disk
prediction of $\nu^{+1/3}$. All these data, although still with quite
low S/N for the other two objects, demonstrate the unique potential of
the technique with future better data. We also present similar data
for other quasars and radio galaxies, and briefly discuss the nature of
the polarization.}
{ Published in MNRAS, 364, 640 }
{E-mail contact: mk@roe.ac.uk,\newline preprint available at
http://arxiv.org/abs/astro-ph/0509341}
\vspace*{0.6cm}
{\large\bf{The Outburst of HST-1 in the M87 Jet}}
{\bf{ D.E. Harris$^1$, C.C. Cheung$^{2,3}$, J.A. Biretta$^4$, W.
Sparks$^4$, W. Junor$^5$, E.S. Perlman$^6$, \& A.S. Wilson$^7$}}
$^1$ {Smithsonian Astrophysical Observatory, 60 Garden St., Cambridge,
MA 02138}\\
$^2$ {Jansky Postdoctoral Fellow; National Radio Astronomy Observatory.
Now hosted by Kavli Institute for Particle Astrophysics and
Cosmology, Stanford University, Stanford, CA 94305}\\
$^3$ {MIT Kavli Institute for Astrophysics \& Space Research, 77
Massachusetts Ave., Cambridge, MA 02139}\\
$^4$ {Space Telescope Science Institute, 3700 San Martin Drive,
Baltimore, MD 21218}\\
$^5$ {Space \& Atmospheric Sciences, Los Alamos National Laboratory,
P.O. Box 1663, Los Alamos, NM 87545}\\
$^6$ {Joint Ctr. for Astrophysics, University of Maryland, Baltimore
County, 1000 Hilltop Circle, Baltimore, MD 21250}\\
$^7$ {Astronomy Department, University of Maryland, College Park,
MD~20742}
{The X-ray intensity of knot HST-1, 0.85$^{\prime\prime}$ from the
nucleus of the radio galaxy M87, has increased by more than a factor of
50 during the last 5 years. The optical increase is similar and our
more limited radio data indicate a commensurate activity. We give the
primary results of our Chandra X-ray Observatory monitoring program and
consider some of the implications of this extreme variability in a
relativistic jet. We find that the data support a 'modest beaming
synchrotron' model as indicated in our earlier papers. Based on this
model, the decay of the X-ray lightcurve appears to be dominated by
light travel time across the emitting region of HST-1, rather than
synchrotron loss timescales.}
{ Accepted by Astrophys. J. }
{E-mail contact: harris@cfa.harvard.edu,\newline preprint available at
http://arxiv.org/abs/astro-ph/0511755}
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{
The Active Galaxies Newsletter is available on the World Wide Web.
You can access it via the University of Manchester home page :-
http://www.ast.man.ac.uk/$\sim$rb/agn/
%%%->>>> http://www.ast.man.ac.uk/~rb/agn/
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If you move or your e-mail address changes, please send the editor
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\begin{document}
\begin{center}
%% If you use any personal Latex commands in your abstract, please include
%% their definitions here.
%% Between these brackets you write the title of your thesis:
{\Large\bf{Title of Thesis}}
\vspace*{0.5cm}
%% Here comes your name
{\bf{ Author }}
%% Here you write the institute where your thesis work was conducted, e.g.:
{Thesis work conducted at: Steward Observatory, University of Arizona, USA}
%% Here comes your present postal address (if you are about to move and know
%% your coming address give it as well) e.g.:
{Current address: European Southern Observatory, Casilla 19001,
Santiago 19, Chile}
%% (if you use this part, remove %%)
%% {Address as of XX XXX 1997: }
%% Here comes your e-mail address:
{Electronic mail: doctor@sun.institute.edu}
%% Name of your adviser:
{Ph.D dissertation directed by: Galileo Galilei}
%% Month and Year of thesis:
{Ph.D degree awarded: Month Year}
\vspace*{0.8cm}
\end{center}
%% Within the following brackets you place your text:
{This is the abstract of your thesis}
\end{document}